Whistler heat flux instability in the solar wind with Bi-Lorentzian velocity distribution functions

Journal Article · Sun May 01 04:00:00 EDT 1977 · J. Geophys. Res.; (United States)

DOI:https://doi.org/10.1029/JA082i013p01889· OSTI ID:7112461

Abraham-Shrauner, B; Feldman, W C

The dependence of the growth rate and the threshold level of the whistler heat flux instability in the solar wind at 1 AU on the shape of the velocity distribution function and on the electron halo temperature anisotropy is examined by using a drifted bi-Lorentzian distribution function. We find that for a given set of plasma parameters the maximum growth rate increases sharply with increasing slope of the halo electron velocity distribution and that the whistler instability threshold level increases sharply with increasing halo temperature anisotropy. In view of the sensitivity of the whistler instability threshold level to details of the shape of halo electron distribution functions it is not now possible to decide unambiguously if the whistler mode regulates the interplanetary heat flux some of the time at 1 AU, but it remains a strong candidate.

• Research Organization: University of California, Los Alamos Scientific Laboratory, Los Alamos, New Mexico 87545
• OSTI ID: 7112461
• Journal Information: J. Geophys. Res.; (United States), Journal Name: J. Geophys. Res.; (United States) Vol. 82:13; ISSN JGREA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
640107 -- Astrophysics & Cosmology-- Planetary Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
DISTRIBUTION FUNCTIONS
ELECTRON TEMPERATURE
HEAT FLOW
INSTABILITY
INSTABILITY GROWTH RATES
INTERPLANETARY SPACE
PLASMA INSTABILITY
SOLAR ACTIVITY
SOLAR WIND
SPACE